%%
%% This is file `sample.bib',
%% generated with the docstrip utility.
%%
%% The original source files were:
%%
%% ubcthesis.dtx  (with options: `samplebib')
%% 
%% This file was generated from the ubcthesis package.
%% --------------------------------------------------------------
%% 
%% Copyright (C) 2001
%% Michael McNeil Forbes
%% mforbes AT alum.mit.edu
%% 
%% (Note that the AT symbol cannot be used in a comment in a bibtex file,
%% hence the lack of a proper email address above.)
%% 
%% This file may be distributed and/or modified under the
%% conditions of the LaTeX Project Public License, either version 1.2
%% of this license or (at your option) any later version.
%% The latest version of this license is in
%%    http://www.latex-project.org/lppl.txt
%% and version 1.2 or later is part of all distributions of LaTeX
%% version 1999/12/01 or later.
%% 
%% This program is distributed in the hope that it will be useful,
%% but WITHOUT ANY WARRANTY; without even the implied warranty of
%% MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE.  See the
%% LaTeX Project Public License for more details.
%% 
%% This program consists of the files ubcthesis.dtx, ubcthesis.ins, and
%% the sample figures fig.eps and fig.fig.
%% 
%% This file may be modified and used as a base for your thesis without
%% including the licence agreement as long as the content (i.e. textual
%% body) of the file is completely rewritten. You must, however, change
%% the name of the file.
%% 
%% This file may only be distributed together with a copy of this
%% program. You may, however, distribute this program without generated
%% files such as this one.
%% 

\ProvidesFile{sample.bib}[2008/05/19 v1.53 ^^J
University of British Columbia Sample Thesis]
%% These are just some examples of articles and books.  Some of the fields
%% are not needed, for example the abstract and SLACcitation fields.  There
%% are many other types of documents.  The entry CL:2000 poses a problem
%% in the URL field.  I am not sure how to get around this right now.

@Article{Forbes:2006ba,
     author    = "Forbes, Michael McNeil and Zhitnitsky, Ariel R.",
     title     = "{Dark antimatter as a galactic heater: X-rays from the core
                  of our  galaxy}",
     journal   = "JCAP",
     volume    = "0801",
     year      = "2008",
     pages     = "023",
     eprint    = "astro-ph/0611506",
     SLACcitation  = "%%CITATION = ASTRO-PH/0611506;%%",
     abstract  = {Several independent observations of the Galactic
       core suggest hitherto unexplained sources of energy.  We
       suggest that dark matter in the form of dense antimatter
       nuggets could provide a natural site for electron and proton
       annihilation, providing 511 {keV} photons, gamma-rays, and
       diffuse {keV} X-ray radiation.  We show that identifying dark
       matter as antimatter nuggets is consistent with the observed
       emissions, and we make definite predictions about their
       spectrum and morphology.  If correct, our proposal not only
       identifies dark matter and explains baryogenesis, but allows
       X-ray observations to directly probe the matter
       distribution in our Galaxy.}
}

@Book{LL3:1977,
  author       = "L. D. Landau and E. M. Lifshitz",
  title        = "Quantum Mechanics: Non-relativistic theory",
  publisher    = "Pergamon Press",
  year         = "1989, c1977",
  volume       = "3",
  series       = "Course of Theoretical Physics",
  address      = "Oxford; New York",
  edition      = "Third",
}

@InCollection{Peccei:1989,
  author       = "R. D. Peccei",
  title        = "Special Topics: The Strong {CP} Problem",
  booktitle    = "CP violation",
  publisher    = "World Scientific",
  year         = "1989",
  editor       = "C. Jarlskog",
  address      = "Singapore",
  month        = jan,
}

@Article{Bulgac:2006gh,
  author =       {Aurel Bulgac and Michael McNeil Forbes and Achim
                  Schwenk},
  title =        {Induced {P-wave} Superfluidity in Asymmetric Fermi
                  Gases},
  journal =      "Phys. Rev. Lett.",
  volume =       97,
  year =         2006,
  pages =        020402,
  eprint =       {arXiv:cond-mat/0602274},
  SLACcitation = "%%CITATION = COND-MAT 0602274;%%",
  abstract =     {We show that two new intra-species P-wave superfluid
                  phases appear in two-component asymmetric Fermi
                  systems with short-range {S-wave} interactions. In
                  the {BEC} limit, phonons of the molecular {BEC}
                  induce {P-wave} superfluidity in the excess
                  fermions. In the {BCS} limit, density fluctuations
                  induce {P-wave} superfluidity in both the majority
                  and the minority species. These phases may be
                  realized in experiments with spin-polarized Fermi
                  gases.}
}

@InProceedings{CL:2000,
  author       = "S. A. {Colgate} and H. {Li}",
  title        = "The Magnetic Fields of the Universe and Their Origin",
  booktitle    = "10 pages, 1 figure (figures.png), invited talk at IAU
                 195 Preprint no. LAUR 00-180.",
  year         = "2000",
  month        = jan,
  pages        = "1418",
  URL          = "{http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=\
2000astro.ph..1418C&db_key=PRE}",
  adsnote      = "Provided by the NASA Astrophysics Data System",
  eprint       = "astro-ph/0001418",
  abstract     = "Recent rotation measure observations of a dozen or so
                 galaxy clusters have revealed a surprisingly large
                 amount of magnetic fields, whose estimated energy and
                 flux are, on average, {$\sim 10^{58}$} ergs and {$\sim
                 10^{41}$ G cm$^2$}, respectively. These quantities are
                 so much larger than any coherent sums of individual
                 galaxies within the cluster that an efficient galactic
                 dynamo is required. We associate these fields with
                 single AGNs within the cluster and therefore with all
                 galaxies during their AGN phase. Only the central,
                 massive black hole (BH) has the necessary binding
                 energy, {$\sim 10^{61}$} ergs. Only the accretion disk
                 during the {BH} formation has the winding number,
                 {$\sim 10^{11}$} turns, necessary to make the gain and
                 magnetic flux. We present a model of the BH accretion
                 disk dynamo that might create these magnetic fields,
                 where the helicity of the {$\alpha - \Omega$} dynamo is
                 driven by star-disk collisions. The back reaction of
                 the saturated dynamo forms a force-free field helix
                 that carries the energy and flux of the dynamo and
                 redistributes them within the clusters.",
}

@Misc{Turner:1999,
  author       = "M. S. Turner",
  title        = "Dark Matter, Dark Energy and Fundamental Physics",
  howpublished = "astro-ph/9912211",
  year         = "1999",
  month        = dec,
  abstract     = "More than sixty years ago Zwicky made the case that
                 the great clusters of galaxies are held together by the
                 gravitational force of unseen (dark) matter. Today, the
                 case is stronger and more precise: Dark, nonbaryonic
                 matter accounts for {$30\% \pm 7\%$} of the critical mass
                 density, with baryons (most of which are dark)
                 contributing only {$4.5\% \pm 0.5\%$} of the critical
                 density. The large-scale structure that exists in the
                 Universe indicates that the bulk of the nonbaryonic
                 dark matter must be cold (slowly moving particles). The
                 SuperKamiokande detection of neutrino oscillations
                 shows that particle dark matter exists, crossing an
                 important threshold. Over the past few years a case has
                 developed for a dark-energy problem. This dark
                 component contributes about {$80\% \pm 20\%$} of the critical
                 density and is characterized by very negative pressure
                 {$(p_X < -0.6 \rho_X)$}. Consistent with this picture of
                 dark energy and dark matter are measurements of {CMB}
                 anisotropy that indicate that total contribution of
                 matter and energy is within {$10\%$} of the critical
                 density. Fundamental physics beyond the standard model
                 is implicated in both the dark matter and dark energy
                 puzzles: new fundamental particles (e.g., axion or
                 neutralino) and new forms of relativistic energy (e.g.,
                 vacuum energy or a light scalar field). A flood of
                 observations will shed light on the dark side of the
                 Universe over the next two decades; as it does it will
                 advance our understanding of the Universe and the laws
                 of physics that govern it.",
}

@Book{Vilenkin:1994,
  author =       {Alexander Vilenkin and E. P. S. Shellard},
  title =        {Cosmic Stringas and Other Topological Defects},
  publisher =    {Cambridge University Press},
  year =         1994,
  address =      {Cambridge}
}

\endinput
%%
%% End of file `sample.bib'.
